Coherent light production found in very low optical density atomic clouds

No atom is an island, and scientists have known for decades that groups of atoms form communities that “talk” to each other. But there is still much to learn about how atoms — particularly energetically excited ones — interact in groups.

In a study published in PRX Quantum, physicists from the University of Wisconsin–Madison observed communication between atoms at lower and lower densities. They found that the atoms influence each other at 100 times lower densities than probed before, exhibiting slow decay rates and emitting coherent light.

“It seems that (low-density) groups of excited atoms spontaneously organize to then produce light that is coherent,” says David Gold, a postdoctoral fellow in Deniz Yavuz’s group and lead author of the study. “These findings are pretty interesting from a basic science standpoint, and in terms of quantum computing, the takeaway is that even with very low numbers of atoms, you can see significant amounts of (these effects).”

A well-established property of atoms is found in electron excitation: when a specific wavelength of light hits an atom of a specific element, an electron is excited to a higher orbital level. As that electron decays back to its initial state, a photon of a specific wavelength is emitted. A single atom has a characteristic decay rate for that process. When groups of atoms are studied, their interactions are observed: the initial decay rate is very fast, or superradiant, then transitions to a slower, or subradiant, rate.

A schematic of the experimental setup. (Top) the overall apparatus used. (A) shows the setup for the first part of the experiment, where the researchers were measuring decay rates in lower and lower density clouds. (B) shows the setup for the second part of the paper, with the addition of an interferometer

Though well-established in dense clouds, this group-talk has never been studied in less dense clouds of atoms, which could have impacts on applications such as quantum computing.

In their first set of experiments, Gold and colleagues asked what the decay rate of lower-density clouds looked like. They supercooled the atoms in a cloud, hit them with an excitation laser, and recorded the decay rates as an intensity of emitted light over time. They observed the characteristic subradiance. In this case, they did not always see superradiance, likely due to the reduced number of atoms available to measure.

profile picture of David Gold
David Gold

Next, they asked what happened if they let the cloud expand — or decrease in density — for varying periods of time before repeating their experiment. They found that as the cloud become less and less dense, the amount of subradiance decreased, until eventually a density was reached where the atoms stopped behaving like a group and instead displayed single-atom decay rates.

“The most subradiance that we observed was at around a hundred times lower optical density than it had previously been observed before,” Gold says.

Now that the researchers knew that a less dense cloud still decays subradiantly to a point, they asked if the decay was happening in an isolated manner, or if the atoms were really acting as a group. If acting as a group, the emitted light would be coherent, or more laser-like, with some structure between the atoms.

They used the same experimental setup but added an interferometer, where light is split and recombined before the photons are detected. They first set the baseline interference pattern by moving the mirror closer or further away from the splitter — changing the path length of one of the beams — and mapping the interference pattern of the split light waves that were emitted from the same atom.

If there were no relationship between the two atoms and the light they emit, then they would have expected to see no interference pattern. Instead, they saw that for some distance of mirror displacement, the lightwaves did interfere, indicating that different atoms being measured were nonetheless producing coherent light.

“I think this is the more exciting thing we found: that the light that’s being emitted is coherent and it has more of the properties of a laser than you would expect,” Gold says. “The atoms are influenced by each other and not in a way we would have expected.”

Aside from the interesting physics seen in the study, Gold says the work is also applicable to quantum computing, particularly as those computers grow bigger in the future.

“Even if everything in a quantum computer is running perfectly and the system was completely isolated, there’s still this inherent thing of, well, the atoms just might decay down from [the computational] state,” Gold says.

This work was supported by National Science Foundation (NSF) Grant No. 2016136 for the QLCI center Hybrid Quantum Architectures and Networks.

Physics technology shines at Summerfest Tech

profile photo of Kieran Furlong
Kieran Furlong

Six top technologies in development at the University of Wisconsin-Madison and other UW System campuses headlined WARF Innovation Day at Summerfest Tech June 29. Wednesday’s event at BMO Tower in Milwaukee drew dozens of in-person and virtual investors who heard seven-minute pitch presentations on high-tech innovations ranging from fusion power to bridge safety monitoring.

“This forum was an exceptional opportunity for investors, media and the public to interface with top University of Wisconsin ideas,” said Erik Iverson, CEO of WARF. “It is this exchange of passion and expertise that forwards the state’s innovation ecosystem.”

One of the presenters included Kieran Furlong, an Honorary Fellow with the College of Letters & Science and CEO of Realta Fusion. Furlong is also the Technology-to-Market (T2M) Advisor to the WHAM project, a fusion energy project led by physics professor Cary Forest.

Furlong’s presentation, titled “Breakthrough Physics for Clean Energy Generation,” had this summary:

The Wisconsin High-field Axisymmetric Mirror (WHAM) project is leveraging major advances in superconducting magnets and plasma heating to pursue commercially viable nuclear fusion power. Fusion is how energy is generated in the sun, yet it has been tremendously challenging to harness on Earth. This project seeks to pave the way to a comparatively low-cost fusion device that can be a net energy generator.

ACCESS THE PITCH DECK.

Read the original article by WARF

Sign up to watch the video on the Summerfest Tech virtual platform.

Brian Rebel promoted to full professor

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Brian Rebel

The Department of Physics is happy to announce that Professor Brian Rebel has been promoted to full professor.

Rebel is a high energy experimentalist whose research focuses on accelerator-based neutrino physics. He joined the department as an associate professor with a joint appointment at Fermilab in 2018, where he is now a senior scientist.

“Professor Rebel is a leader in neutrino science, making major contributions to DUNE experiments and having published recently on four different neutrino collaborations,” says Mark Eriksson, physics department chair. “The department is thrilled about his promotion to full professor.”

Rebel has established himself as a leader in the Long-Baseline Neutrino Facility (LBNF) and Deep Underground Neutrino Experiment (DUNE). DUNE is an international experiment for neutrino science and proton decay studies that consists of two neutrino detectors — one near Fermilab in Illinois, and one in South Dakota. The experiment will be installed in LBNF, which will produce the neutrino beam. Rebel is currently the DUNE Anode Plane Assembly (APA) consortium manager, and has previously led Fermilab’s DUNE Science Group.

Since 2005, Rebel has also been involved in Fermilab’s NOvA experiment, which uses precision measurements to investigate the flavor oscillations of neutrinos that are not predicted by the Standard Model. He is currently serving as the co-convener of the analysis group searching for oscillations of active neutrino flavors into a sterile neutrino.

Rebel is currently training three graduate students and two postdoctoral scholars, and expects to graduate his first UW–Madison doctoral student soon. Additionally, he supervised several trainees at Fermilab before he came to UW–Madison. He has enjoyed teaching both introductory physics as well as physics courses for non-majors, and is an effective and engaging teacher.

Congrats, Prof. Rebel, on this well-deserved recognition!

 

 

NASA Sounding Rocket Mission Seeks Source of X-rays Emanating From Inner Galaxy

This post was originally published by NASA

To human eyes, the night sky between the stars appears dark, the void of space. But X-ray telescopes capture a profoundly different view. Like a distant firework show, our images of the X-ray sky reveal a universe blooming with activity. They hint at yet unknown cosmic eruptions coming from somewhere deeper into our galaxy.

To help find the source of these mysterious X-rays, University of Wisconsin—Madison astronomer Dan McCammon and his team are launching the X-ray Quantum Calorimeter or XQC instrument. XQC will make its seventh trip to space aboard a NASA suborbital rocket. This time, XQC will observe a patch of X-ray light with 50 times better energy resolution than ever before, key to revealing its source. The launch window opens at Equatorial Launch Australia’s Arnhem Space Centre in Northern Territory, Australia, on June 26, 2022.

Because Earth’s atmosphere absorbs X-rays, our first views of cosmic X-rays awaited the space age. In June 1962, physicists Bruno Rossi and Ricardo Giacconi launched the first X-ray detector into space. The flight revealed the first sources of X-rays beyond our Sun: Scorpius X-1, a binary star system some 9,000 light-years away, as well as a diffuse glow spread across the sky. The discovery founded the field of X-ray astronomy and later won Giacconi a share of the 2002 Nobel Prize in physics.

a heatmap of the night sky that is mostly blue but has a few blobs of green and warmer colors like orange and red. One of the blobs is circled, indicating the area that McCammon's team is focusing on
This image shows a “map” of the night sky in soft X-ray light in galactic coordinates, with the Sun positioned at the center. The horizontal line across the middle of the image runs along the plane of our disk-shaped galaxy. University of Wisconsin, Madison astronomer Dan McCammon and the XQC team will be observing the bright blob in the center of the image, circled with a dotted line. This is the southern part of a roughly circular blob around the center of the galaxy, cut in half by cold absorbing gas in the plane of the galaxy.
Credits: Snowden et al., 1997

Scientists have now mapped the X-ray sky in ever-finer detail with the help of other NASA X-ray missions. Still, there are several bright patches whose sources are unknown. For the upcoming flight, McCammon and his team will target a patch of X-ray light only partly visible from the Northern Hemisphere.

“It covers a big part of the galaxy, but we needed to be in the Southern Hemisphere to see that part of the sky,” McCammon said. “We’ve been waiting a long time for this expedition to Australia.”

Scientists believe the X-ray patch comes from diffuse, hot gas heated by supernovae, the brilliant eruptions of dying stars. The XQC mission is investigating two possible sources, illustrated in the graphic below.

One possibility is that the X-rays come from gas heated by “Type Ia” supernovae, the death throes of massive stars that live tens to hundreds of millions of years. The inner part of our galaxy has a high enough concentration of this type of supernova to heat the X-ray patch McCammon is investigating.

The other possible source is “Type II” supernovae. The stars behind Type II supernova are even more massive, burn brighter and hotter, and live just a few million years before going supernova. They occur in active star-forming regions, like those in one of our galaxy’s inner spiral arms.

To distinguish these possibilities, XQC will analyze the X-ray light, looking for traces of oxygen and iron. More oxygen points to Type II supernovae, while less oxygen suggests Type 1a supernovae. The physics behind it is complex but ultimately stems from how long the stars burned before erupting. The smaller stars behind Type 1a supernovae burn for longer, leaving less oxygen behind than Type II supernovae.

Of course, the flight is likely to capture much more information as well. “This is an exploration with a new capability – we want to see what we can see,” McCammon said. “Every time we look at the X-ray sky with a new capability, it turns out to be more complicated that we supposed.”

After the flight, the team plans to recover the instrument. It will retire to Oak Ridge National Labs in Tennessee where it will aid in laboratory experiments.

This flight will be XQC’s final trip to space, but the very first from the new Arnhem Space Centre rocket range in East Arnhem, Australia. XQC is part of a three-rocket campaign launching from the range in June and July 2022, NASA’s first time launching from Australia since 1995.

Sau Lan Wu honored with named planet

The International Astronomical Union (IAU) has named a minor planet ‘Saulanwu’ after UW–Madison physics professor Sau Lan Wu.

The planet (177770) ‘Saulanwu’ (=2005 JE163) was discovered on May 8, 2005 at Mt Lemmon observatory in southern Arizona by a NASA funded project, the Catalina Sky Survey. More details about the planet can be found from NASA’s JPL website, including a sketch of the planet’s orbit, which is in the asteroid belt between Mars and Jupiter. Minor planet ‘Saulanwu’ is about two kilometers in diameter, and it takes four years to orbit the sun once. This planet is relatively stable, dynamically, and is expected to remain in our cosmos for millions of years to come.

Wu was nominated for this honor by astronomer Gregory J. Leonard from the University of Arizona’s Department of Planetary Sciences.

a certificate announcing that Sau Lan Wu has had a minor planet named after her

Victor Brar, Moritz Münchmeyer funded through latest round of Research Forward

Victor Brar

Sixteen projects — including two from Physics — have been selected for funding in the second round of Research Forward, a program to stimulate innovative and groundbreaking research at UW–Madison that is collaborative, multidisciplinary and potentially transformative.

The winning projects were chosen from 96 proposals submitted by applicants across campus. The Research Forward initiative is sponsored by the Office of the Vice Chancellor for Research and Graduate Education and is supported by the Wisconsin Alumni Research Foundation, which provides funding for one or two years, depending on the needs and scope of the project. Some of the projects that have been funded have the potential to fundamentally transform a field of study.

profile photo of Moritz Muenchmeyer
Moritz Münchmeyer

The Research Forward initiative is sponsored by the Office of the Vice Chancellor for Research and Graduate Education and is supported by the Wisconsin Alumni Research Foundation, which provides funding for one or two years, depending on the needs and scope of the project. Some of the projects that have been funded have the potential to fundamentally transform a field of study.

“Research Forward encourages collaboration among campus PIs, enhances PhD student and postdoc training, and strengthens our external grant funding requests,” says Steve Ackerman, vice chancellor for research and graduate education. “The projects we selected are truly forward-looking and use innovative approaches and tools such as state-of-the-art machine learning methods, 3D printing techniques and geostationary satellites.”

The Physics projects are:

Keith Bechtol selected to Department of Energy Early Career Research Program

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Keith Bechtol

The Department of Energy’s (DOE) Office of Science announced the selection of 83 scientists — including University of Wisconsin–Madison physics professor Keith Bechtol — to the Early Career Research Program.

The funding will allow Bechtol and his group to first work on commissioning the Vera C. Rubin Observatory in preparation for the Legacy Survey of Space and Time (LSST), then they will transition to data collection and analysis for their cosmology research.

“We are anticipating that LSST will catalog more stars, more galaxies and more solar system objects during its first year of operations than all previous telescopes combined,” Bechtol says.

Rubin Observatory’s telescope will have an eight-meter diameter mirror and a ten square degree field of view. The 3.2-billion-pixel camera will collect an image every 30 seconds. All told, LSST will amass around 10 terabytes of data every night.

Bechtol has leadership roles for building and commissioning the observatory as well as with the Dark Energy Science Collaboration (DESC), the international science collaboration that will make high accuracy measurements of fundamental cosmological parameters using LSST data. At least seven other collaborations have formed around different science areas to analyze the data. Rubin Observatory is preparing to serve the LSST data to many thousands of scientists in the US, Chile, and at international partner institutions around the world.

“DESC will use LSST data to address several outstanding physics questions, such as: Why are the distances between galaxies growing at an accelerating rate? What is the fundamental nature of dark matter? What is the absolute mass scale of neutrinos? How did the universe begin and what were the initial conditions?” Bechtol says.

Bechtol will receive around $150,000 per year for five years to cover summer salary and research expenses. The research expenses will be used mostly to cover the analyses after the data collection starts. However, because there cannot be useful data without the initial commissioning and science validation steps — and because the Observatory is still a couple of years away from first light — the DOE award is also supporting Bechtol’s efforts during the commissioning phase to accelerate the realization of DESC science goals.

“For me, the most important thing about this award is that it will provide more opportunity for students and postdocs to directly contribute to this ambitious experiment. Turning on a new experiment of this scale and complexity doesn’t happen every day,” Bechtol says. “For my research group to be able to participate firsthand in the commissioning, seeing first light, and contributing to the first cosmology results is so valuable from a career development perspective. We are training the next generation of experiment builders.”

The DOE early career program is open to untenured, tenure-track professors at a U.S. academic institution (or a full-time employee at a DOE national laboratory) who received a PhD within the past 10 years. Research topics are required to fall within one of the DOE Office of Science’s eight major program offices, including high energy physics, the program through which Bechtol’s award was made.

 

Thad Walker honored with Vilas Distinguished Achievement Professorship

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Thad Walker

Extraordinary members of the University of Wisconsin–Madison faculty, including physics professor Thad Walker, have been honored during the last year with awards supported by the estate of professor, U.S. senator and UW Regent William F. Vilas (1840-1908).

Walker was one of seventeen professors were named to Vilas Distinguished Achievement Professorships, an award recognizing distinguished scholarship as well as standout efforts in teaching and service. The professorship provides five years of flexible funding — two-thirds of which is provided by the Office of the Provost through the generosity of the Vilas trustees and one-third provided by the school or college whose dean nominated the winner.

In addition, nine professors received Vilas Faculty Mid-Career Investigator Awards and six professors received Vilas Faculty Early Career Investigator Awards.

Detailed analysis of old star provides template for heavy element formation

This story was originally published by University Communications

The fusion furnaces that are the universe’s stars create the elements from helium up to iron. But iron is only number 26 on the periodic table out of well over 100 known elements. So the heavier ones, like gold, lead and uranium, must come from somewhere other than fusion.

Scientists have long known that those heavy elements come from neutron capture, where neutrons are added to an element that make it unstable, then it radioactively decays and its atomic number increases by one. Nearly 70 years ago, they confirmed one site, or event, of a neutron capture method known as the slow, or s-process. The rapid, or r-process, was not confirmed with a site until 2017, when the LIGO/VIRGO collaboration detected a neutron star merger.

“With a neutron star merger, the neutron stars are ripped apart and they throw out neutrons, and you can build lots of heavy elements out of these neutron stars,” says Jim Lawler, a professor of physics at the University of Wisconsin–Madison. “The mystery arises when we look at the total r-process inventory of our home galaxy: Can we explain all that with neutron star mergers or are there additional sites?”

In a new study led by astronomers from the University of Michigan, Lawler and colleagues identified the elemental composition of HD 222925, a Milky Way star located over 1400 lightyears from earth. Their analysis confirmed that the star was rich in r-process elements, and they were able to identify and calculate the relative abundance of each element. They also found that the star is iron- and metal-poor, a proxy for age that indicates HD 222925 is relatively old and provides information about early star formation.

“We were able to determine a complete r-process abundance pattern for what we think is probably one event that happened early in the beginning of the universe,” Lawler says. “So that r-process template now can be used to screen various models of the nuclear physics that produce the r-process and see if the models for all sites are physically correct.”

At UW–Madison, Lawler and scientist Elizabeth Denhartog contributed the spectroscopic analysis that identified the elements in the star. Every element has a unique electromagnetic spectrum that can be separated into spectral lines using a diffraction grating — just like a prism separates white light into a rainbow. HD 222925 is a relatively bright star, meaning it provided stronger spectra to analyze. It was also identified by the Hubble Space Telescope, providing access to data in the ultraviolet range that is normally blocked by the ozone layer and undetectable by telescopes on Earth.

For the full story, read more on the University of Michigan’s news site.

THIS STUDY WAS SUPPORTED IN PART BY NASA (GRANTS GO-15657, GO-15951, AND 80NSSC21K0627); U.S. NATIONAL SCIENCE FOUNDATION (NSF, GRANTS PHY 14-30152, OISE 1927130, AST 1716251 AND AST 1815403); AND THE U.S. DEPARTMENT OF ENERGY (GRANT DE-FG02-95-ER40934); AND NOIRLAB, WHICH IS MANAGED UNDER A COOPERATIVE AGREEMENT WITH THE NSF.

Researchers aim X-rays at century-old plant secretions for insight into Aboriginal Australian cultural heritage

This story was originally published by David Krause at SLAC

For tens of thousands of years, Aboriginal Australians have created some of the world’s most striking artworks. Today their work continues long lines of ancestral traditions, stories of the past and connections to current cultural landscapes, which is why researchers are keen on better understanding and preserving the cultural heritage within.

close up of a tall, narrow, spiky brown plant
Secretions called exudate cover parts of the spike of a Xanthorrhoea plant — colloquially called “grass tree” or “yakka” — used in aboriginal art. PHOTO COURTESY FLINDERS UNIVERSITY, SOUTH AUSTRALIA

In particular, knowing the chemical composition of pigments and binders that Aboriginal Australian artists employ could allow archaeological scientists and art conservators to identify these materials in important cultural heritage objects. Now, researchers are turning to X-ray science to help reveal the composition of the materials used in Aboriginal Australian cultural heritage – starting with the analysis of century-old samples of plant secretions, or exudates.

Aboriginal Australians continue to use plant exudates, such as resins and gums, to create rock and bark paintings and for practical applications, such as hafting stone points to handles. But just what these plant materials are made of is not well known.

Therefore, scientists from six universities and laboratories around the world turned to high-energy X-rays at the Stanford Synchrotron Radiation Lightsource (SSRL) at the Department of Energy’s SLAC National Accelerator Laboratory and the synchrotron SOLEIL in France. The team aimed X-rays at ten well-preserved plant exudate samples from the native Australian genera EucalyptusCallitrisXanthorrhoea and Acacia. The samples had been collected more than a century ago and held in various institutions in South Australia.

The results of their study were clearer and more profound than expected.

“We got the breakthrough data we had hoped for,” says Uwe Bergmann, physicist at the University of Wisconsin–Madison and former SLAC scientist who develops new X-ray methods. “For the first time, we were able to see the molecular structure of a well-preserved collection of native Australian plant samples, which might allow us to discover their existence in other important cultural heritage objects.”

Researchers today published their results in the Proceedings of the National Academy of Sciences.

Profile picture of Uwe Bergmann
Uwe Bergmann

Looking below the surface

Over time, the surface of plant exudates can change as the materials age. Even if these changes are just nanometers thick, they can still block the view underneath it.

“We had to see into the bulk of the material beneath this top layer or we’d have no new information about the plant exudates,” SSRL Lead Scientist Dimosthenis Sokaras says.

Conventionally, molecules with carbon and oxygen are studied with lower-energy, so-called “soft” X-rays, that would not be able to penetrate through the debris layer. For this study, researchers sent high-energy X-ray photons, called “hard” X-rays, into the sample. The photons squeezed past foggy top layers and into the sample’s elemental arrangements beneath. Hard X-rays don’t get stuck in the surface, whereas soft X-rays do, Sokaras says.

Once inside, the high-energy photons scattered off of the plant exudate’s elements and were captured by a large array of perfectly aligned, silicon crystals at SSRL. The crystals filtered out only the scattered X-rays of one specific wavelength and funneled them into a small detector, kind of like how a kitchen sink funnels water drops down its drain.

Next, the team matched the wavelength difference between the incident and scattered photons to the energy levels of a plant exudate’s carbon and oxygen, providing the detailed molecular information about the unique Australian samples.

5 brown glass jars with pigment samples outside of them
Century-old plant exudate samples in amber jars. Researchers mapped the chemistries of these samples using high-energy photons, knowledge that will help study and preserve the work of aboriginal artists who used plant material. PHOTO COURTESY FLINDERS UNIVERSITY, SOUTH AUSTRALIA

A path for the future

Understanding the chemistries of each plant exudate will allow for a better understanding of identification and conservation approaches of Aboriginal Australian art and tools, Rafaella Georgiou, a physicist at Synchrotron SOLEIL, said.

“Now we can go ahead and study other organic materials of cultural importance using this powerful X-ray technique,” she says.

Researchers hope that people who work in cultural heritage analysis will see this powerful synchrotron radiation technique as a valuable method for determining the chemistries of their samples.

“We want to reach out to that scientific community and say, ‘Look, if you want to learn something about your cultural heritage samples, you can come to synchrotrons like SSRL,’” Bergmann says.

SSRL is a DOE Office of Science user facility. In addition to SSRL, parts of this research were carried out at SOLEIL in France and three CNRS laboratories (PPSM, IPANEMA, IMPMC). The University of Pisa, the Université Paris-Saclay, the University of Melbourne, Flinders University, the Australian Synchrotron International Synchrotron Access Program, and other organizations also supported this research.